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Perspectives on Gamma-Ray Burst Physics and Cosmology with Next Generation Facilities

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journal contribution
posted on 12.10.2016, 12:11 by Weimin Yuan, Lorenzo Amati, John K. Cannizzo, Bertrand Cordier, Neil Gehrels, Giancarlo Ghirlanda, Diego Götz, Nicolas Produit, Yulei Qiu, Jianchao Sun, Nial R. Tanvir, Jianyan Wei, Chen Zhang
High-redshift Gamma-Ray Bursts (GRBs) beyond redshift (Formula presented.) are potentially powerful tools to probe the distant early Universe. Their detections in large numbers and at truly high redshifts call for the next generation of high-energy wide-field instruments with unprecedented sensitivity at least one order of magnitude higher than the ones currently in orbit. On the other hand, follow-up observations of the afterglows of high-redshift GRBs and identification of their host galaxies, which would be difficult for the currently operating telescopes, require new, extremely large facilities of at multi-wavelengths. This chapter describes future experiments that are expected to advance this exciting field, both being currently built and being proposed. The legacy of Swift will be continued by SVOM, which is equipped with a set of space-based multi-wavelength instruments as well as and a ground segment including a wide angle camera and two follow-up telescopes. The established Lobster-eye X-ray focusing optics provides a promising technology for the detection of faint GRBs at very large distances, based on which the THESEUS, Einstein Probe and other mission concepts have been proposed. Follow-up observations and exploration of the reionization era will be enabled by large facilities such as SKA in the radio, the 30 m class telescopes in the optical/near-IR, and the space-borne WFIRST and JWST in the optical/near-IR/mid-IR. In addition, the X-ray and (Formula presented.)-ray polarization experiment POLAR is also introduced.

History

Citation

Space Science Reviews, 2016, December 2016, 202 (1), pp. 235–277

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

AM (Accepted Manuscript)

Published in

Space Science Reviews

Publisher

Springer Verlag

issn

0038-6308

eissn

1572-9672

Acceptance date

29/06/2016

Copyright date

2016

Available date

21/07/2017

Publisher version

http://link.springer.com/article/10.1007/s11214-016-0274-z

Notes

The file associated with this record is under a 12 month embargo from publication in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.

Language

en

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